Journal Article

The close classical T Tauri binary V4046 Sgr: complex magnetic fields and distributed mass accretion

J.-F. Donati, S. G. Gregory, T. Montmerle, A. Maggio, C. Argiroffi, G. Sacco, G. Hussain, J. Kastner, S. H. P. Alencar, M. Audard, J. Bouvier, F. Damiani, M. Güdel, D. Huenemoerder and G. A. Wade

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 417, issue 3, pages 1747-1759
Published in print November 2011 | ISSN: 0035-8711
Published online October 2011 | e-ISSN: 1365-2966 | DOI:
The close classical T Tauri binary V4046 Sgr: complex magnetic fields and distributed mass accretion

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We report here the first results of a multi-wavelength campaign focusing on magnetospheric accretion processes within the close binary system V4046 Sgr, hosting two partly convective classical T Tauri stars of masses ≃0.9 M and age ≃12 Myr. In this paper, we present time-resolved spectropolarimetric observations collected in 2009 September with ESPaDOnS at the Canada–France–Hawaii Telescope (CFHT) and covering a full span of 7 d or ≃2.5 orbital/rotational cycles of V4046 Sgr. Small circularly polarized Zeeman signatures are detected in the photospheric absorption lines but not in the accretion-powered emission lines of V4046 Sgr, thereby demonstrating that both system components host large-scale magnetic fields weaker and more complex than those of younger, fully convective classical T Tauri stars (cTTSs) of only a few Myr and similar masses.

Applying our tomographic imaging tools to the collected data set, we reconstruct maps of the large-scale magnetic field, photospheric brightness and accretion-powered emission at the surfaces of both stars of V4046 Sgr. We find that these fields include significant toroidal components, and that their poloidal components are mostly non-axisymmetric with a dipolar component of 50–100 G strongly tilted with respect to the rotation axis; given the similarity with fields of partly convective main-sequence stars of similar masses and rotation periods, we conclude that these fields are most likely generated by dynamo processes. We also find that both stars in the system show cool spots close to the pole and extended regions of low-contrast, accretion-powered emission; it suggests that mass accretion is likely distributed rather than confined in well-defined high-contrast accretion spots, in agreement with the derived magnetic field complexity.

Keywords: techniques: polarimetric; stars: formation; stars: imaging; stars: individual: V4046 Sgr; stars: magnetic fields; stars: rotation

Journal Article.  9576 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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